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We present a comprehensive X-ray study of the neutron star low-mass X-raybinary IGR J17062-6143, which has been accreting at low luminosities since itsdiscovery in $2006$. Analysing NuSTAR, XMM-Newton and Swift observations, weinvestigate the very faint nature of this source through three approaches:modelling the relativistic reflection spectrum to constrain the accretiongeometry, performing high-resolution X-ray spectroscopy to search for anoutflow, and searching for the recently reported millisecond X-ray pulsations.We find a strongly truncated accretion disk at $77^{+22}_{-18}$ gravitationalradii ($\sim 164$ km) assuming a high inclination, although a low inclinationand a disk extending to the neutron star cannot be excluded. Thehigh-resolution spectroscopy reveals evidence for oxygen-rich circumbinarymaterial, possibly resulting from a blueshifted, collisionally-ionised outflow.Finally, we do not detect any pulsations. We discuss these results in thebroader context of possible explanations for the persistent faint nature ofweakly accreting neutron stars. The results are consistent with both anultra-compact binary orbit and a magnetically truncated accretion flow,although both cannot be unambigiously inferred. We also discuss the nature ofthe donor star and conclude that it is likely a CO or O-Ne-Mg white dwarf,consistent with recent multi-wavelength modelling.

The very-faint X-ray binary IGR J17062-6143: a truncated disk, no pulsations and a possible outflow